| URBANCOVÁ, Gabriela, Martin URBANEC, Oliver HAMIL and Jiřina ŘÍKOVSKÁ STONE. Braking index of isolated pulsars. Physical Review D. US - Spojené státy americké, 2015, vol. 91, No 6, p. "063007-1"-"063007-9", 9 pp. ISSN 1550-7998. Available from: https://dx.doi.org/10.1103/PhysRevD.91.063007. |
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@article{43081,
author = {Urbancová, Gabriela and Urbanec, Martin and Hamil, Oliver and Říkovská Stone, Jiřina},
article_location = {US - Spojené státy americké},
article_number = {6},
doi = {http://dx.doi.org/10.1103/PhysRevD.91.063007},
keywords = {rotating relativistic stars; braking index; equation of state},
language = {eng},
issn = {1550-7998},
journal = {Physical Review D},
title = {Braking index of isolated pulsars},
url = {http://journals.aps.org/prd/abstract/10.1103/PhysRevD.91.063007},
volume = {91},
year = {2015}
}
TY - JOUR
ID - 43081
AU - Urbancová, Gabriela - Urbanec, Martin - Hamil, Oliver - Říkovská Stone, Jiřina
PY - 2015
TI - Braking index of isolated pulsars
JF - Physical Review D
VL - 91
IS - 6
SP - "063007-1"-"063007-9"
EP - "063007-1"-"063007-9"
SN - 15507998
KW - rotating relativistic stars
KW - braking index
KW - equation of state
UR - http://journals.aps.org/prd/abstract/10.1103/PhysRevD.91.063007
N2 - Isolated pulsars are rotating neutron stars with accurately measured angular velocities Omega, and their time derivatives that show unambiguously that the pulsars are slowing down. Although the exact mechanism of the spin-down is a question of detailed debate, the commonly accepted view is that it arises through emission of magnetic dipole radiation (MDR) from a rotating magnetized body. The calculated energy loss by a rotating pulsar with a constant moment of inertia is assumed proportional to a modeldependent power of Omega. This relation leads to the power law (Omega) over dot = -K Omega^n where n is called the braking index. The aim of this work is to determine the deviation of the value of n from the canonical n = 3 for a star with a frequency dependent moment of inertia in the region of frequencies from zero (static spherical star) to the Kepler velocity (onset of mass shedding by a rotating deformed star), in the macroscopic MDR model. We use microscopic realistic equations of
ER -
URBANCOVÁ, Gabriela, Martin URBANEC, Oliver HAMIL and Jiřina ŘÍKOVSKÁ STONE. Braking index of isolated pulsars. \textit{Physical Review D}. US - Spojené státy americké, 2015, vol.~91, No~6, p.~''063007-1''-''063007-9'', 9 pp. ISSN~1550-7998. Available from: https://dx.doi.org/10.1103/PhysRevD.91.063007.
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